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1 Flow, Turbulence and Combustion 63: , Kluwer Academic Publishers. Printed in the Netherlands. 443 Reynolds Number Dependence of Energy Spectra in the Overlap Region of Isotropic Turbulence STEPHAN GAMARD and WILLIAM K. GEORGE Department of Mechanical and Aerospace Engineering, State University of New York, Buffalo, NY 14260, U.S.A. Abstract. A Near-Asymptotics analysis of the turbulence energy spectrum is presented that accounts for the effects of finite Reynolds number recently reported by Mydlarski and Warhaft [21]. From dimensional and physical considerations (following Kolmogorov and von Karman), proper scalings are defined for both low and high wavenumbers, but with functions describing the entire range of the spectrum. The scaling for low wavenumbers uses the kinetic energy and the integral scale, L, based on the integral of the correlation function. The fact that the two scaled profiles describe the entire spectrum for finite values of Reynolds number, but reduce to different profiles in the limit, is used to determine their functional forms in the overlap region that both retain in the limit. The spectra in the overlap follow a power law, E(k) = Ck 5/3+µ,whereµ and C are Reynolds number dependent. In the limit of infinite Reynolds number, µ 0andC constant, so the Kolmogorov/Obukhov theory isrecovered inthe limit.explicitexpressions forµ and the other parameters are obtained, and these are compared to the Mydlarski/Warhaft data. To get a better estimate of the exponent from the experimental data, existing models for low and high wavenumbers are modified to account for the Reynolds number dependence. They are then used to build a spectral model covering all the range of wavenumbers at every Reynolds number. Experimental data from grid-generated turbulence are examined and found to be in good agreement with the theory and the model. Finally, from the theory and data, an explicit form for the Reynolds number dependence of φ = εl/u 3 is obtained. Key words: energy spectrum, isotropic, overlap region, near asymptotics, energy decay, Reynolds number effect. 1. Introduction In 1941 Kolmogorov [15] introduced his ideas for the similarity of small scale turbulence and the inertial subrange. This was subsequently extended to the energy spectrum by Obukhov [22] who first derived the famous k 5/3 -law. In spite of the modifications by Kolmogorov himself [16], and apart from recent questions about universality, for more than fifty years this theory has been widely discussed and more or less accepted. An often overlooked assumption in Kolmogorov s theory, however, is the necessity of a sufficiently large Reynolds number before the assumptions can be expected to hold. This qualification is especially relevant since there are few spectral measurements which unequivocally show a k 5/3 spectral

2 444 S. GAMARD AND W.K. GEORGE range. And even those were made at very high Reynolds numbers, well above those for which the theory is commonly applied. In 1996, Mydlarski and Warhaft [21] proposed, on experimental grounds, that the exponent in the inertial subrange in fact was not the 5/3 proposed by Kolmogorov, but rather a function of the Reynolds number that perhaps went to 5/3 in the limit of infinite Reynolds number. For all the Reynolds numbers of their experiments, the spectrum rolled-off more slowly than k 5/3 ; moreover, the lower the Reynolds number the greater the difference. As noted above, there have been numerous theoretical attempts to modify the exponent in the power law, first suggested by Kolmogorov [16] himself, mostly to account for internal intermittency (see [4] for a review). But these deviations from the k 5/3 behavior can not explain the Mydlarski and Warhaft observations, since all arguments for internal intermittency cause the spectrum to roll-off faster than k 5/3, not slower. Recently George [6, 8] (see also [9]) proposed two ideas which allow treatment of finite Reynolds number effects in turbulent flows when infinite Reynolds number forms of the equations are available. The first is the Asymptotic Invariance Principle (AIP) which states that properly scaled solutions at infinite Reynolds number must be similarity solutions to the limiting equations themselves. Thus the determination of scaling parameters is determined by the equations themselves, not by ad hoc arguments. The second is the methodology of Near-Asymptotics which provides a means to find overlap solutions at finite Reynolds number when inner and outer forms of the limiting equations are available. These ideas were successfully applied to a number of wall-bounded turbulent flows. This paper theoretically justifies Mydlarski and Warhaft s conclusions by applying the AIP and Near-Asymptotics to the spectral energy equation for isotropic turbulence. The results will be seen to be in remarkable agreement with the data, thereby providing additional confirmation from the governing equations for both the experiments and the methodology. An interesting (and perhaps even surprising) outcome of this work will be an analytical expression for the Reynolds number dependence of the important ratio L/l = εl/u 3 where L is the physical integral scale. 2. Theoretical Analysis 2.1. BASIC EQUATIONS AND DEFINITIONS Following Batchelor [2], we will use the energy spectrum function, E(k,t),defined by integrating the energy tensor ii over spherical shells of values k, i.e., E(k,t) = 1 2 ii (k) dσ(k), (1) k= k

3 REYNOLDS NUMBER DEPENDENCE OF ENERGY SPECTRA 445 where dσ(k) is an element of surface in wavenumber space at radius k = k, and ii is the trace of the Fourier transform of the two-point velocity correlation tensor given by ij (k) = 1 8π 3 e ik r u i (x)u j (x + r) dr. (2) Note that E(k,t) is a scalar function of only the magnitude k = k, hence the directional information has been removed. Also, hereafter the time-dependence of E will be suppressed and it will be written simply as E(k). The integral of E over all wavenumbers k yields the turbulence energy: 3 2 u2 = 1 2 u iu i = 0 E(k)dk. (3) The rate of dissipation of turbulent kinetic energy per unit mass (or simply the dissipation rate), ε, is related to the energy spectrum by ε = 2ν 0 k 2 E(k)dk. (4) For isotropic turbulent flow the energy equation reduces to a balance among simply the time rate of change of the energy spectrum, E/ t, the energy transfer between different wavenumbers, T, and the viscous dissipation, 2νk 2 E, i.e., E(k) = T(k) 2νk 2 E(k). (5) t The energy spectrum typically rises from zero at k = 0toapeakvalueata wavenumber near the inverse of the integral scale defined below, then rolls-off for higher wavenumbers. Hence the energy is dominated by wavenumbers around the peak. Viscous stresses dominate the highest wavenumbers and make the primary contribution to the dissipation integral THE LENGTH SCALES The Integral Length Scale There exists much confusion about which scales are really appropriate to the description of the energy spectrum at large scales. We shall refer to the large scale we consider most important as the physical integral scale, L, and define it from the integral of the longitudinal velocity correlation:

4 446 S. GAMARD AND W.K. GEORGE Longitudinal integral scale: L 1 u u 1 (x,y,z,t)u 1 (x + r, y, z, t) dr. (6) For isotropic turbulence, L can equivalently be obtained from the energy spectrum function as: L = 3π 0 E(k)/k dk 4 0 E(k)dk. (7) Thus, L is completely determined once E(k) is given. It is important to note that the physical integral scale differs from the pseudo integral scale (l u 3 /ε) often found in the literature (and used by Mydlarski and Warhaft as well). It will be argued below that the ratio L/l = φ is Reynolds number dependent and constant only in the limit of infinite Reynolds number; i.e., L l = εl φ(r). (8) u The Kolmogorov Microscale The other important length scale of importance to the analysis presented below is the Kolmogorov microscale, η. Using Kolmogorov s second hypothesis which implies that the only parameters in the equilibrium range in the infinite Reynolds number limit are ε and the viscosity ν, it follows that the length scale is given by: ( ν 3 ) 1/4 η =. (9) ε This scale is characteristic of the high wavenumber part of the spectrum since it is of the order of the smallest eddies found in homogeneous turbulence The Reynolds Number We define a Reynolds number, R, based on the ratio of the length scales given by: R = L η. (10) Note that this differs from the definition of Reynolds number of R l = ul/ν used in many texts (cf. [26]). Here R l = (R/φ(R)) 4/3.

5 REYNOLDS NUMBER DEPENDENCE OF ENERGY SPECTRA SIMILARITY CONSIDERATIONS Similarity Scalings for Low and High Wavenumbers A dimensional analysis of the energy spectrum shows its proportionality to the product of a length and the square of a characteristic velocity. Following Batchelor, it has been customary to scale the spectrum in two ways: Low wavenumber (or energy variables) using u and L (or l); say k = kl, f L (k,r) = E(k,t) u 2 L. (11) High wavenumber (or Kolmogorov variables) using η, u η (νε) 1/4 ; say k + = kη, f H (k +,R) = E(k,t) u 2 η η = E(k,t). (12) ε 1/4 ν5/4 The first form of Equation (11) was originally suggested by von Karman and Howarth [27], while the latter was first proposed by Obukhov [22]. Note that it is commonly assumed that the Kolmogorov scale collapses the spectral data at high wavenumbers, regardless of the Reynolds number. This cannot be exactly the case, however, since the whole idea of an equilibrium range in the spectrum at high wavenumbers is predicated on the separation of scales [2]. The Kolmogorov scaling can at most represent an infinite Reynolds number limit to which finite Reynolds number spectra asymptote as the turbulent Reynolds number increases. Thus, regardless of which set of parameters the spectrum is scaled by, either retain a Reynolds number dependence for finite values of R. It is this weak (and asymptotically vanishing) dependence on Reynolds number which is explored in the analysis below, and which will be seen to be responsible for the observations of Mydlarski and Warhaft [21]. It is important to note that both f L and f H represent exactly the same spectrum since, at least at finite Reynolds number, they are just different nondimensionalizations of the same function. Because of this it follows immediately that: f L (k, R) = R 5/3 φ 2/3 f H (k +,R). (13) In the limit of infinite Reynolds number however, f H becomes independent of R and loses the ability to describe the low wavenumber spectral behavior. Similarly

6 448 S. GAMARD AND W.K. GEORGE f L becomes independent of R but loses the ability to describe the dissipation range. But both retain an inertial subrange in the limit, a k 5/3 range which extends to infinity for the low wavenumber scaled forms and to zero for the high. This has long been recognized and is represented in most texts (cf. [26]). This can be argued in a slightly different way. In the limit of infinite Reynolds number f L and f H are similarity solutions of different limiting forms of Equation (5). (This is straightforward to show by substituting the low and high wavenumber scaled versions of Equations (11) and (12) in Equation (5), and carrying out the limit as R.) For finite values of k, the low wavenumber form reduces in the limit to a simple balance between the temporal decay and the spectral transfer to the high wavenumbers, say ε k. The high wavenumber form reduces to the familiar local equilibrium range [2], where there is simply a balance between the dissipation and the spectral transfer from the low wavenumbers, but this is just ε k. Since all of the energy dissipated in this limit must come via the spectral flux from low wavenumbers, then ε k = ε (but only in the limit). Thus for the low wavenumbers in the limit of infinite Reynolds number, the only parameters are the energy, u 2 and the dissipation, ε. And for the high wavenumbers the only parameters are the dissipation, ε, and the kinematic viscosity, ν. Hence u 2 and ε alone govern the low wavenumber spectrum exactly in the limit, while ν and ε alone govern exactly the high. Thus in the limit of infinite Reynolds number, both the von Karman/Howarth and Kolmogorov scalings become exact and independent of Reynolds number, i.e., lim f L(k,R) = f L (k) only, R and lim f H (k +,R)= f H (k + ) only. R This is, of course, the whole idea behind scaling in the first place; namely that the spectra should collapse, at least in the limit. And in this case they do since they are similarity solutions to equations which themselves become independent of the Reynolds number in the limit as R = L/η. This is, in fact, the Asymptotic Invariance Principle of George [8]. Obviously f L (k) and f H (k + ) can not have the same functional dependence on k, except possibly in an overlap region (the so-called inertial subrange). In fact, as is well known, at low wavenumbers, f H k + 5/3 while for high wavenumbers f L k 5/3 [26]. It will be seen to be possible below using the methodology of Near-Asymptotics to extend this reasoning to finite Reynolds numbers, and deduce the Mydlarski and Warhaft results from first principles without additional assumptions.

7 REYNOLDS NUMBER DEPENDENCE OF ENERGY SPECTRA MATCHING OF THE TWO PROFILES The low and high wavenumber spectra have been scaled with different scales. But the ratio of those scales is Reynolds number dependent. Therefore, at finite Reynolds numbers, there cannot exist any region in which either scaling is truly Reynolds number independent. Note that this does not mean the scaled spectra will not collapse approximately, only that perfect collapse can be achieved only in the limit. It is this lack of perfect collapse at finite Reynolds numbers which is the key to understanding the analysis below. Now as long as we consider only finite Reynolds numbers, f L (k, R) and f H (k +,R) represent the spectrum for all wavenumbers. It is only in the limit as R that f L loses the ability to describe the high wavenumbers and f H the low. The traditional asymptotic matching begins with the limiting forms, f L and f H, and tries to stretch their region of validity to match them in an overlap region (if such a region exists). Such an analysis for the energy spectra is presented in [26], and the resulting matched region is the k 5/3 -region, or inertial subrange. If, however, we consider the finite Reynolds number forms instead of the limiting ones, the problem of solving the overlap region can be approached in a different way. Since both f L and f H already describe the entire spectrum, there is no need to stretch their range of validity and match them. They already match perfectly at all wavenumbers, but have simply been scaled differently. Instead, our problem is that these finite Reynolds number functions degenerate in different ways at infinite Reynolds number, one losing high wavenumbers, the other the low. Our objective is to use this information to determine their functional form in the remaining common region they describe in this limit (if it exists). This methodology is known as Near-Asymptotics and was first developed in [8] (see also [9, 10]). In the following paragraphs it is applied to the energy spectrum. Even if we do not know the analytical forms of f L and f H, we can still use their properties. Both describe the same spectrum, so they must satisfy u 2 Lf L (k, R) = (ε ν 5 ) 1/4 f H (k +,R). (14) Equivalently, using the definition of R = L/η and defining φ = εl u, (15) 3 we can write f L (k, R) = R 5/3 φ 2/3 f H (k +,R). (16) The function φ(r) is the ratio of the physical integral scale, L, to the pseudointegral scale, l = u 3 /ε. The Kolmogorov reasoning summarized above implies that φ constant in the limit as R. As noted earlier, it is only in this limit that L and l can be used interchangeably. To simplify the following expressions, we define g as g(r) = R 5/3 φ 2/3. (17)

9 REYNOLDS NUMBER DEPENDENCE OF ENERGY SPECTRA 451 Since the first term on the right-hand side is a function of R only, we define γ(r)by γ(r) R dg g dr and S L and S H by S L (k, R) ln f L(k, R) ln R S H (k +,R) ln f H (k +,R) ln R = d(ln g) dlnr, (25), (26) k k +. (27) Now Equation (24) can be written as k f L f L k = k+ f H R f H k + = γ(r)+[s H (k +,R) S L (k,r)]. (28) R As noted earlier, in the limit as R, both f L and f H become asymptotically independent of R, each losing in the process the ability to describe part of the spectrum. Thus, from the definitions of S L and S H, the term in square brackets in Equation (28) must vanish identically. This leaves only the first term which must go to a constant, i.e., k f L k + f H lim = lim R f L k R f H k + = lim γ(r) γ. (29) R R R So there is indeed a common part which survives in this limit. We shall see below that the constant, γ = 5/3, so the Kolmorogov/Obukhov result is obtained as the infinite R limit. The question of most interest, however, is: what happens at large but finite Reynolds numbers? In other words, is there any wavenumber region where k f L = k+ f H f L k f H k + γ(r), (30) R R even when γ(r) γ > 0? If so, we have found the explanation for the Mydlarski and Warhaft results. To examine this, we look how S L and S H are changing with ln R. A Taylor expansion about a given value of R at fixed k yields: S L (k, R) f L(k, R + R) f L (k,r) f L (k,r) R R, (31)

10 452 S. GAMARD AND W.K. GEORGE and S H (k +,R) f H (k +,R+ R) f H (k +,R) R f H (k +,R) R. (32) Thus S L and S H represent the relative Reynolds number dependencies of f L and f H. They must, of course, vanish in the limit of infinite Reynolds number since the scaled spectra are similarity solutions to the limiting equations. At finite Reynolds numbers, S L goes from near zero for small values of k where the low wavenumber scaling is approximately correct, and increases as k becomes large since the low wavenumber scaling does apply at the dissipative scales. For S H, it is just the opposite, large for small k + and decreasing toward zero as k + approaches infinity. The whole question of whether there is an overlap region at finite Reynolds number then reduces to whether there is a common region where S H S L γ(r). Another possibility would be that S L = S H, namely that both scaling profiles have the same R dependence. We shall assume there is such a region, and show this leads to a consistent approximation. Therefore, we neglect (S H S L ) relative to γ(r)and write simply k f L = γ(r), (33) f L k R k + f H f H k + = γ(r). (34) R The solutions to these equations must be recognized as first-order approximations only, the higher order contributions having been neglected. They do, however, reduce to the correct limiting solutions, and retain at least that Reynolds number dependent part of the solution which is independent of wavenumber. The neglect of S H S L must be and can be justified a posteriori. Integrating Equations (33) and (34) leads immediately to Reynolds number dependent power laws for both f L and f H, i.e., f L (k, R) = C L (R) (k) γ(r), (35) f H (k +,R) = C H (R) (k + ) γ(r). (36) Substituting the definition of g (Equation (17)) into Equation (25) yields γ = 5/3 + µ, (37) where µ has been defined to be µ = 2 dlnφ 3 dlnr. (38) Note since φ constant as R,thisimpliesthatµ 0 in the same limit. But this in turn implies that γ = 5/3, which yields immediately the result obtained by Obukhov [22], as noted above.

11 REYNOLDS NUMBER DEPENDENCE OF ENERGY SPECTRA 453 By using Equation (18), we can express g as: g(r) = f L = C L(R) f H C H (R) R 5/3+µ(R). (39) Substituting γ(r)= 5/3 + µ from Equation (25) into Equation (39) shows that a solution is possible only if ln R dγ dlnr = dlnc H /C L dlnr. (40) This equation makes it clear that µ, C H and C L are inter-related, and cannot simply be chosen arbitrarily. Also, it is easy to show that satisfying this constraint insures that S H S L 0 for the overlap solution, consistent with the original hypothesis. Like µ, C H /C L can also be shown to be simply related to φ(r). Comparing Equations (17) and (39), it follows immediately that C H = φ 2/3 R µ(r). (41) C L We know from the Kolmogorov argument presented above that φ φ where φ is an non-zero constant. Also C H and C L must be finite and different from zero in the limit of infinite Reynolds number; otherwise the scaled spectra would either go to zero or increase without bound. But this is not physically possible, since they must represent exact similarity solutions of the governing equations in the limit of infinite Reynolds number. (In other words, the scaling itself would have to be wrong.) Taking the logarithm of Equation (41) yields ln C H = 2 ln φ + µ ln R. (42) C L 3 It follows immediately that both C H /C L and φ can be non-zero constants in the limit as R only if µ 0 faster than 1/ ln R! Thus, everything about the Reynolds number dependence is contained in the unknown function, φ(r). Ifφ can be determined, all our functions will be known. Alternatively, if C H /C L is determined, then so is φ. Even the determination of µ allows φ to be expressed to within an integration constant. This latter possibility is the approach followed below. It may seem surprising that the Reynolds number dependence of the overlap region is intimately linked to the Reynolds number dependence of φ = εl/u 3. As noted above, however, the asymptotic constancy of φ depends crucially on the Kolmogorov argument relating the spectral flux in the inertial subrange to the exact dissipation. Therefore it should not be surprising that these break down together at finite Reynolds number. Nor should it be surprising that a theory which accounts for the Reynolds number dependence of one, also accounts for the other. All of the conditions can be satisfied in two ways: This immediately rules out the conjecture of Barenblatt and Chorin [1] who take µ 1/ ln R.

12 454 S. GAMARD AND W.K. GEORGE Possibility 1 (Reynolds number independent overlap range): φ constant, and µ = 0 and the overlap region is Reynolds number independent. Or φ must satisfy two conditions as ln R ; namely: Possibility 2 (Reynolds number dependent overlap range): Condition 1. φ φ = constant. Condition 2. µ = (2/3)d ln φ/d ln R 0 faster than 1/ ln R. The first possibility leads to a 5/3 power-law which is independent of Reynolds number. Mydlarski and Warhaft [21] have shown, however, that the exponent of real data is Reynolds number dependent. Therefore it is the Reynolds number dependent solution of Possibility 2 that is of primary interest here. 3. The Function µ The function µ can be completely determined only with a closure model for the turbulence. In the absence of that, we must resort to empirical forms. Even so, we know a great deal about its behavior. First, it is clear from Equation (40) that µ will be most naturally expressed in terms of the argument ln R. Second, Condition 1 above can be satisfied only if µ depends on inverse powers of ln R. In fact, if we expand about the infinite Reynolds number limit, µ must be asymptotically of the form: βa [ µ(ln R) = 1 + a + ] 1, (43) (ln R) 1+β ln R where the constant βa is chosen of this form for convenience later. Note that Condition 2 can be satisfied only if β>0. The consequences of failing to satisfy either condition are that similarity cannot be maintained in the overlap region. Clearly this would be unphysical since both the low and high wavenumber scalings are similarity solution to the energy equation in the limit. George and Castillo [9] and George et al. [10] were successful by truncating Equation (43) at the first term. We shall do the same here, i.e., βa µ =, (44) (ln R) 1+β where the only adjustable parameters are A and β. It follows immediately from Equation (38) that ln φ = 3A φ 2(ln R). (45) β

15 REYNOLDS NUMBER DEPENDENCE OF ENERGY SPECTRA 457 For isotropic turbulence L = L 1 = 2L 2, a condition not exactly satisfied by the data, but easily dealt with as we shall show later. The values of ε were determined by integrating the one-dimensional spectral data and using ε = ε 1 + 2ε 2 where ε α is defined by: ε α = 5 0 k 2 1 F 1 αα (k 1) dk 1. (58) 4.2. THE HIGH WAVENUMBER SCALING The one-dimensional spectral data in high wavenumber variables is shown in Figure 1. This is the classical Kolmogorov scaling (Equation (12)), and has been shown to be reasonably successful at high wavenumbers in many experiments. Such is the case here. As expected, the scaled spectra clearly separate at low wavenumbers where the scaling in no longer appropriate. This behavior with Reynolds number of the spectrum at low wavenumbers is also expected (cf. [26]), and is a direct consequence of the arguments presented previously. Note that, contrary to expectations, there is not a consistent trend with Reynolds numbers at low wavenumbers. This perhaps can be attributed to the difference between the initial conditions for the various grids THE LOW WAVENUMBER SCALING The low wavenumber scaling (Equation (11)) needs the integral scale for the one-dimensional half-line spectrum. Only the pseudo-integral scale was used by Mydlarski and Warhaft who took l = 0.9u 3 /ε. Therefore, a determination of L 1 and L 2 was essential. The spectra can not be determined at zero wavenumbers, of course, because of record length limitations. Moreover, the spectral errors cannot be removed by the usual smoothing since there are fewer estimates at these low wavenumbers. The one-dimensional spectra at the origin (k 1 = 0) can be expanded, however, as F 1 11 = A 1 B 1 k C 1 k 4 1, (59) F 1 22 = A B 2 k 2 1, (60) where B 1 = B 2 if the turbulence is isotropic [26]. By fitting the curves to the measured spectra at the lowest wavenumbers, it was possible to extrapolate to zero wavenumber values without being dependent on simply the lowest wavenumber data alone. The values of the different integral scales are presented in Table I. The integral scales do not satisfy the isotropic relations. Therefore, we plotted the longitudinal spectra using F11 1 /u2 1 L 1 versus k 1 L 1 ; and the lateral spectra as

17 REYNOLDS NUMBER DEPENDENCE OF ENERGY SPECTRA 459 Figure 2. One-dimensional spectra in low wavenumber scaling. F 1 22 /u2 2 L 2 versus k 1 L 2. As shown in Figure 2, both show a good collapse except for the high wavenumbers where the scaling is no longer appropriate. The lack of a consistent Reynolds numbers trend at high wavenumbers outside the collapse zone is also present here, just as for the high wavenumber scaling. Figure 3 shows the same spectra non-dimensionalized with u and l = 0.9u 3 /ε, the pseudo-integral scale used by Mydlarski and Warhaft. Although the differences are slight, the physical integral scale L 1 (or L 2 ) is the better choice. Note that either L or l could have been used in the analysis above, but the results obtained using L are more useful since the Reynolds number dependence of the ratio L/l appears explicitly in µ instead of in S H S L.

18 460 S. GAMARD AND W.K. GEORGE Figure 3. One-dimensional spectra scaled with u and l, the pseudo-integral scale DETERMINATION OF µ, C H AND C L FROM THE DATA Figure 4 illustrates the Mydlarski and Warhaft conclusions quite simply. When the spectrum is multiplied by k + 5/3, none of the spectra show the flat region implied by a 5/3 power law. This is consistent with our theory, both that the power is not 5/3 for any of the data, and that this value can at most be approached asymptotically. Nonetheless, there is always some subjectivity in the determination of µ. Mydlarski and Warhaft [21] chose the best exponent, n, to enable k n 1.F 1 αα to achieve a constant plateau. (Note that n = 5/3 + µ.) They did not, however, utilize the isotropic properties of their spectra; and thus, cited two different values

19 REYNOLDS NUMBER DEPENDENCE OF ENERGY SPECTRA 461 Figure 4. One-dimensional spectra in high wavenumber scaling multiplied by k + 5/3 1. for µ: one for the longitudinal part of the spectrum and one for the lateral part. In our analysis of the same data, we treated the longitudinal and lateral spectra together using the isotropic conditions above. This, in effect, doubles the amount of data that can be used and reduces the statistical error. Two different methods were applied to the data to obtain independent estimates of the parameters µ, C H, and C L (and from them A and β in Equation (44)): Method 1 begins with plots in inner and outer variables of and k 1 F11 1 df 1 11 dk 1, (61) k 1 F22 1 df 1 22 dk 1, (62) where the derivatives were computed directly from the data. It is easy to show that in the power law region (if there is one) these are equal to 5/3 + µ. A typical result is illustrated in Figure 5. Once µ is found in this manner, the values of C Hα and C Lα are read on the curves of F + 1 αα (k+ 1) 5/3 µ and F 1 αα (k 1) 5/3 µ, similar to the approach of Mydlarski and Warhaft. Method 2 was developed to deal with the fact that both of the above methods have difficulty distinguishing unambiguously precisely what data should be included in

20 462 S. GAMARD AND W.K. GEORGE Figure 5. Derivation of µ using (k + /f H )( f H / k + ) = 5/3 + µ(r) for R λ = 473. the overlap region. This is because both the low and high wavenumber regions have some residual influence on it, especially at the lowest Reynolds numbers. This is a common problem in applying any asymptotic theory to real data, and is illustrated by Figure 6 which plots the result of applying Method 2 to the high and low wavenumber semi-empirical spectral models discussed in the Appendix. Also plotted is the composite spectrum obtained by multiplying them together and dividing by the common part. (These spectral models are discussed in detail in the Appendix to avoid interrupting the main theme of this paper.) While the high wavenumber model asymptotes to k 5/3+µ at low wavenumbers, and the low to the same at high wavenumbers, their product never achieves this value exactly like the real data!

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